The Martian nakhlite meteorites, ormed from a single magma source region, and emplaced during multiple events spanning at least 93 ± 12 Ma, represent a key opportunity to study the evolution of Martian volcanic petrogenesis. Here 16 of the 26 identified nakhlite specimens are studied using coupled large area electron backscatter diffraction (EBSD) and energy dispersive X-ray spectroscopy (EDS) mapping to determine shape preferred orientation (SPO) textures of contained augite (high Ca-clinopyroxene) phenocrysts by considering crystallographic preferred orientation (CPO). Textural parameters derived from EBSD and EDS analyses were used to calculate maximum and minimum magma body crystallization thicknesses via three endmember emplacement scenarios: thermal diffusion, crystal settling, and crystal convection. Results from CPO textural analyses indicate weak to moderate fabric textures that are comparable to those in terrestrial clinopyroxenites. In all samples, a consistent foliation within the {001} axis of augite is observed. In all but two of the studied nakhlites this {001} foliation is typically coupled with a weaker lineation fabric in one or more of the {100}, {010}, {001} axes. Results from the calculated magma body thicknesses are consistent with an emplacement mechanism for the nakhlites driven by crystal settling. These crystal settling results infer magmatic body thicknesses ranging from <1 m to several 10’s m, forming two distinguishable groups that appear random when assessed against observed texture, geochemical, and age parameters. Coupled textural and modelling results therefore suggest that the nakhlite source volcano varied in thickness over time yet consistently solidified via the mechanism of crystal settling.